Searches for Continuous Gravitational Waves from 15 Supernova Remnants and Fomalhaut b with Advanced LIGO

Creators: Abbott, B. P.; Abbott, R.; Adhikari, R. X.; Ananyeva, A.; Anderson, S. B.; Appert, S.; Arai, K.; Araya, M. C.; Barayoga, J. C.; Barish, B. C.; Billingsley, G.; Biscans, S.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Brunett, S.; Cahillane, C.; Callister, T. A.; Coughlin, M. W.; Couvares, P.; Coyne, D. C.; Ehrens, P.; Eichholz, J.; Etzel, T.; Feicht, J.; Gossan, S. E.; Grassia, P.; Gustafson, E. K.; Heptonstall, A. W.; Hulko, M.; Isi, M.; Kamai, B.; Kanner, J. B.; Kasprzack, M.; Kondrashov, V.; Korth, W. Z.; Kozak, D. B.; Lazzarini, A.; Lo, R. K. L.; Markowitz, A.; Maros, E.; Massinger, T. J.; Matichard, F.; McIver, J.; Meshkov, S.; Pedraza, M.; Quintero, E. A.; Reitze, D. H.; Richardson, J. W.; Robertson, N. A.; Rollins, J. G.; Sachdev, S.; Sanchez, E. J.; Sanchez, L. E.; Sun, L.; Taylor, R.; Torrie, C. I.; Trudeau, R. J.; Vajente, G.; Vass, S.; Venugopalan, G.; Wade, A. R.; Wallace, L.; Weinstein, A. J.; Willis, J. L.; Wipf, C. C.; Xiao, L.; Yamamoto, H.; Zhang, L.; Zucker, M. E.; Zweizig, J.; Barkett, K.; Chen, Y.; Li, X.; Ma, Y.; Pang, B.; Scheel, M.; Tso, R.; Varma, V.; LIGO Scientific Collaboration; Virgo Collaboration

Abstract

We describe directed searches for continuous gravitational waves (GWs) from 16 well-localized candidate neutron stars, assuming none of the stars has a binary companion. The searches were directed toward 15 supernova remnants and Fomalhaut b, a directly imaged extrasolar planet candidate that has been suggested to be a nearby old neutron star. Each search covered a broad band of frequencies and first and second time derivatives. After coherently integrating spans of data from the first Advanced LIGO observing run of 3.5–53.7 days per search, applying data-based vetoes, and discounting known instrumental artifacts, we found no astrophysical signals. We set upper limits on intrinsic GW strain as strict as 1 × 10^(−25), fiducial neutron star ellipticity as strict as 2 × 10^(−9), and fiducial r-mode amplitude as strict as 3 × 10^(−8).

Additional Information

© 2019. The American Astronomical Society. Received 2019 January 4; revised 2019 March 7; accepted 2019 March 18; published 2019 April 23. The authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO, as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS), and the Foundation for Fundamental Research on Matter, supported by the Netherlands Organisation for Scientific Research, for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies, as well as by the Council of Scientific and Industrial Research of India; the Department of Science and Technology, India; the Science & Engineering Research Board (SERB), India; the Ministry of Human Resource Development, India; the Spanish Agencia Estatal de Investigación; the Vicepresidència i Conselleria d'Innovació Recerca i Turisme and the Conselleria d'Educació i Universitat del Govern de les Illes Balears; the Conselleria d'Educació Investigació Cultura i Esport de la Generalitat Valenciana; the National Science Centre of Poland; the Swiss National Science Foundation (SNSF); the Russian Foundation for Basic Research; the Russian Science Foundation; the European Commission; the European Regional Development Funds (ERDF); the Royal Society; the Scottish Funding Council; the Scottish Universities Physics Alliance; the Hungarian Scientific Research Fund (OTKA); the Lyon Institute of Origins (LIO), the Paris Île-de-France Region; the National Research, Development and Innovation Office Hungary (NKFIH); the National Research Foundation of Korea; Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation; the Natural Science and Engineering Research Council Canada; the Canadian Institute for Advanced Research; the Brazilian Ministry of Science, Technology, Innovations, and Communications; the International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR); the Research Grants Council of Hong Kong; the National Natural Science Foundation of China (NSFC); the Leverhulme Trust; the Research Corporation; the Ministry of Science and Technology (MOST), Taiwan; and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS, and State of Niedersachsen/Germany for provision of computational resources. This paper has been assigned document No. LIGO-P1800333. Data files for the figures are available at https://dcc.ligo.org/P1800333/public. Software: LALSuite (LIGO Scientific Collaboration 2018).

Errata

B. P. Abbott et al 2021 ApJ 918 91

Attached Files

Published - Abbott_2019_ApJ_875_122.pdf

Submitted - 1812.11656.pdf

Erratum - Abbott_2021_ApJ_918_91.pdf

Files

Abbott_2021_ApJ_918_91.pdf

Files (5.4 MB)

Name	Size	Download all
Abbott_2021_ApJ_918_91.pdf md5:d60720fac7d1267b8d1590b40715780b	457.9 kB	Preview Download
1812.11656.pdf md5:daf51645c56a28f791d28be92f2b0743	2.9 MB	Preview Download
Abbott_2019_ApJ_875_122.pdf md5:82d297c435eaac977c1dcc7de60fe187	2.0 MB	Preview Download

Additional details

	All versions	This version
Views	0	0
Downloads	0	0
Data volume	0 Bytes	0 Bytes